Hostname: page-component-586b7cd67f-2brh9 Total loading time: 0 Render date: 2024-11-23T23:16:37.207Z Has data issue: false hasContentIssue false
  • English
  • Français

Molecular Composition of Local Dwarf Galaxies: Astrochemistry in Low-metallicity Environments

Published online by Cambridge University Press:  30 October 2019

Yuri Nishimura ,
Takashi Shimonishi ,
Yoshimasa Watanabe ,
Nami Sakai ,
Yuri Aikawa ,
Akiko Kawamura ,
Kotaro Kohno  and
Satoshi Yamamoto
Yuri Nishimura
Affiliation:
Institute of Astronomy, The University of Tokyo email: [email protected] Chile Observatory, National Astronomical Observatory of Japan
Takashi Shimonishi
Affiliation:
Frontier Research Institute for Interdisciplinary Sciences, Tohoku University Astronomical Institute, Tohoku University
Yoshimasa Watanabe
Affiliation:
Faculty of Pure and Applied Sciences, University of Tsukuba Tomonaga Center for the History of the Universe, University of Tsukuba
Nami Sakai
Affiliation:
RIKEN
Yuri Aikawa
Affiliation:
Department of Astronomy, The University of Tokyo
Akiko Kawamura
Affiliation:
Chile Observatory, National Astronomical Observatory of Japan
Kotaro Kohno
Affiliation:
Institute of Astronomy, The University of Tokyo email: [email protected]
Satoshi Yamamoto
Affiliation:
Research Center for the Early Universe, The University of Tokyo
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

To investigate molecular composition of low-metallicity environments, we conducted spectral line survey observations in the 3 mm band toward three dwarf galaxies, the Large Magellanic Cloud, IC 10, and NGC 6822 with the Mopra 22 m, the Nobeyama 45 m and the IRAM 30 m, respectively. The rotational transitions of CCH, HCN, HCO+, HNC, CS, SO, 13CO, and 12CO were detected in all three galaxies. We found that the spectral intensity patterns are similar to one another regardless of star formation activities. Compared with Solar-metallicity environments, the molecular compositions of dwarf galaxies are characterized by (1) deficient nitrogen-bearing molecules and (2) enhanced CCH and suppressed CH3OH. These are interpreted (1) as a direct consequence of the lower elemental abundance of nitrogen, and (2) as a consequence of extended photon dominated regions in cloud peripheries due to the lower abundance of dust grains, respectively.

Keywords

galaxies: dwarfgalaxies: ISMISM: cloudsradio lines: galaxiesastrochemistry
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 182 - 185
Copyright
© International Astronomical Union 2019 

References

Bresolin, F., Garnett, D. R., & Kennicutt, R. C. Jr. 2004, ApJ, 615, 228 CrossRefGoogle Scholar
Bolatto, A. D., Jackson, J. M., Wilson, C. D., & Moriarty-Schieven, G. 2000, ApJ, 532, 909 CrossRefGoogle Scholar
Dufour, R., Shields, G., & Talbot, R. Jr 1982, ApJ, 252, 461 CrossRefGoogle Scholar
Esteban, C., García-Rojas, J., Carigi, L., et al . 2014, MNRAS, 443, 624 CrossRefGoogle Scholar
Gao, Y., & Solomon, P. M. 2004, ApJS, 152, 63 CrossRefGoogle Scholar
Garnett, D. R., Edmunds, M. G., Henry, R. B.C., et al . 2004, ApJ, 128, 2772 CrossRefGoogle Scholar
Lequeux, J., Peimbert, M., Rayo, J., Serrano, A., & Torres-Peimbert, S. 1979, A&A, 80, 155 Google Scholar
Magrini, L., & Gonçalves, D. R. 2009, MNRAS, 398, 280 CrossRefGoogle Scholar
Turner, B. 1995, ApJ, 449, 635 CrossRefGoogle Scholar
Turner, B., Pirogov, L., & Minh, Y. 1997, ApJ, 483, 235 CrossRefGoogle Scholar
Turner, B., Herbst, E., & Terzieva, R. 2000, ApJS, 126, 427 CrossRefGoogle Scholar
van der Tak, F., Black, J. H., Schöier, F., Jansen, D., & van Dishoeck, E. F. 2007, A&A, 468, 627 Google Scholar
Watanabe, N., & Kouchi, A. 2002, ApJL, 571, 173 CrossRefGoogle Scholar
Watanabe, Y., Sakai, N., Sorai, K., & Yamamoto, S. 2014, ApJ, 788, 4 CrossRefGoogle Scholar